Strain data after noise subtraction

Several noise sources that are linearly coupled to the GW data channel can be subtracted in post-processing, using
auxiliary sensors (e.g. photodiodes monitoring beam motion).
For LIGO, we remove calibration lines, power mains and harmonics, the effect of some length and angular controls,
and the effect of laser beam motion. This noise removal can improve the sensitivity of the LIGO detectors by
approximately 20%. For Virgo, we remove the effect of some length controls, and the laser
frequency stabilization control.
For reference:

Below are links to strain h(t) time series centered at GPS 1186741861.

The noise subtraction procedure applies a window which tapers the first and last few minutes of the H1 and L1 data files. To remove this corrupt data, the H1 and L1 cleaned data files have been shortened to a total duration of 3584 seconds.